T.Takahashi

Gamma-ray Observation in SpaceSynergy between X-ray and Gamma-ray Observationpresent and future

Tadayuki Takahashi Institute of Space and Astronautical Science (ISAS)

Yasushi FukazawaHiroshima Univ.

Makoto TashiroSaitama Univ.

Astro-E2/Swift/Glast

Astro-E2/Glast

Astro-E2/Swift

GLAST2006

INTEGRAL2002

ChandraNewton

AstroE II

Swift2003

AstroE22005

Compton-GRO Satellite

Astro-E22005

Gamma-ray Mission in 21st Century

AGILE2003

(Makishima et al. 2002)

X-ray/Gamm-ray Observation is crucial

to access Black Hole

JetX-ray

Gamma-ray

Black Hole

・Hot plasmaHigh Temperature

　　electron/Ion

Non-Themal Emission from accelerated Particle

Non-Thermal Emission from the extremelyhigh density/temperature plasma

Hard X-ray & Gamma-ray

Toward the event horizon

To Probe Obscured Black Hole

NGC4945 Done et al. 1996

X-ray/Chandra Komossa et al., 2002

Binary BH in NGC 6240

Optical/HST Van der Marelet al.,2002

N

S

Source of Gravitational Wave?from presentation by G H i (2003)

PKS0528+134

Mkn421

surprise!

Kubo et al. 1997

Gamma-ray Black Hole (Blazars)

The relativistic jet points close to the observer. The non-thermal emission is Doppler boosted and greatly enhanced.

• Synchrotron,peak at IR-X ray energies

• Inverse Compton, peak at GeV-TeV energies

from the same electron distribution

Blazar Variability & Internal Shocks

4/25 4/26 4/27 4/28 4/29 4/30

Time (hours since April 23 1998 23:00 UT )

0 50 100 150

0.5-7.5 keV

• Rfo =0.7, Tchr =40 ks⇒ D 0 =1x1013 cm　　　sG =0.015, G=15 (assumed)• Γ / σΓ =1,000

Simulation Observation

EUVE1keV6.3keV15keV

Lkin ~1,000 LjetTanihata, Takahashi, Kataoka et al. 2002,Iwamoto, Takahara et al. 2003from G. Madejski, 2001

Mrk421

Takahashi et al. 2000

Particle Accelerator in SNRs (1)The remnant of SN 1006

　

CANGAROO TeV Gamma-ray

(Tanimori et al. 1998)

Power-law type spectrum= synchrotron radiation

Discovery of synchrotron X-ray emission by ASCA (Koyama et al. 1995)

X-ray image

I(ε) ∝ε−Γ

Photon indexΓ=3.0

hν synch = 5.3 E100TeV2 B10µG [keV]

Direct evidence of > 10 TeV particles

X-ray observation ⇒ highest energy electrons

X-ray spectrum

Log ε

(from presentationby Uchiyama 2003)

Bamba et al. 2003

Particle Accelerator inSNRs (2)

AcceleratorTarget

Characteristic 1/εSpectrum(Uchiyama, Takahashiand Aharonian,2002)

TeVγ-ray

ASCA

Chandra

molecular cloud

Filament

Emission due to electron/proton interactionin the dense molecular cloud

GeV γ-ray

Annihilation Fountain in the Center of Milky Way

511 keV

CGRO-OSSE

Purcell et al. 1977

Deep Sky: Black holes are ubiquitous in the Universe

Gamma-ray Burst

6 hours 48 hours

Afrerglow:X-ray Images from BeppoSaxBASTE

Optical discoveries of host galaxies and measurements of spectroscopic redshift distances

Gamma Ray bursts are occuring in distant (z = 1-3) galaxies

HST

Most powerful and relativistic phenomena known (1052-1054 ergs)

Present and FutureX-ray/Gamma-ray Missions

I N T E G R A L

Milagro

AGASA, HiRes, A U G E R

Celeste, STACEE

Cangaroo3, VERITAS H E S SMAGIC

AstroE2

OSSECMPTL

HETE2

RXTE, BeppoSAX

Whipple,Cangaroo1/2CAT, HEGRA

EGRET G L A S T

SWIFT

Ene

rgy

in e

V

102

104

106

108

1010

1012

1014

2000 2004 2008 2012 2016

AGILE GeV

MeV

keV

TeV

>PeV

MAXIX M M AstroE2

C h a n d r a

NeXT (Japan)

Constellation X

>1016

Year of Operation Compiled by Kamae (2002)

Electro-Magnetic Radiationand Electron Energy

keV MeV GeV TeV

GLAST(Bremsstrahlung)

Radio Synchrotron

X-ray Brems.X-ray Inv.Compton

GLAST(Inverse Compton)

X-ray Synch.

Electron Energy

Integral Mission (2002-)Big Gamma-ray Mission After CGRO

(15 keV 10 MeV)Imaging (Coded Mask)High Energy ResolutionX-ray Detector (JEM-X)

from Integral Homepage

High resolution Gamma-ray detector (SPI)

19 Cooled Ge detector (each 6x7 cm)FWHM : 2keV @ 1.3 MeV

from Integral Homepage

Solar Flare Spectrum by SPI

from Integral Homepage

(CdTe + CsI(Tl))7 keV @ 100 keV

16384 CdTe detectorstotal area 2620 cm2

with 4x4 mm2 x2mmt detector

IBIS

http://astro.estec.esa.nl/Integral/from Integral Homepage

INTEGRAL Integral Science

osi

44Ti 26Al

1.5 MeV 1.8 MeV

Line Gamma-ray from Nuclear Decay

511 keV Annihilation line from our galaxy

by OSSE

44Ti and 26Al (and more)from past SN explosions Vela region

by Comptel

High Energy and Spatial Resolution

INTEGRAL SPI(Tobs = 106s)

Galactic Plane ScanCen region with ISGR (CdTe Imager)

from Integral Homepage

Swift Mission (2003- )• Multi-wavelength observatory

– Burst Alert Telescope (BAT): 10-150 keV

• detect ~ 300 gamma ray bursts per year• onboard computation of positions• arc-minute positional accuracy

– Dedicated telescopes for X-rays, UV, and optical afterglow follow up:

• 0.3-10 keV X-ray Telescope (XRT)• 170-650 nm UV/Optical Telescope (UVOT)• 0.3-2.5 arc-second locations• existing hardware from JET-X and XMM• determine redshifts from X-ray absorption,

lines, and Lyman-α cutoffRapid response satellite

20 - 70 sec to slew within FOV of BAT

autonomous operations factor 100 improved response timecontinue monitoring of fading afterglow

BAT Imager on Swift•32768 CdZnTe detectors（4x4 mm2 x2mmt detector）• Japanese Contribution to Calibration/Software (ISAS/Saitama U./U. Tokyo)

Multiwavelength Cascade of Images

Gamma Ray (arc-minute)

X-ray (2.5 arc-second)

UVOT (0.3 arc-second)

HST, Keck, etc.

Swift Performance

GRB980228

• Location in host galaxies• Probe the surrounding environment• Use gamma-ray bursts as cosmological probes

Sensitivity

AstroE2 Multi-band Mission

0.5~600100105,000Astro-E

0.3~121012010,000Newton

0.3~100.5120800Chandra

Erage(keV)Δθ

（arcsec)ΔE(e V)Fe 6.7KeV

S(cm2)

Five thin-foil mirrorsFour X-ray CCD cameras(XIS)Microcalorimeter array(XRS)

Non-imaging Hard X-ray detector

AstroE2

Launch 2005 Feb.

XRS

CCD(XIS)

HXD

• Recovery Mission of Astro-E• Launch in 2005• Design almost identical to Astro-E

ISAS

Hard X-ray Detector (HXD)• Narrow FOV

by well type (phoswitch) active shield& passive fine collimator

(<100keV)• Wide energy band (10 – 600 keV)

w/ 64 Si-PIN (2mm thick) diodes• Background rejection

w/ LSI pulse shape discriminationanti-coincidence with 36 detector units

& onboard CPU softwareLow Background & High sensitivity are expected

passive fine collimator (FOVFWHM~30’)

BGO active shield/Well type collimator (FOV~4deg)

GSO detection crystal

Si-PIN diode

ISAS, U.Tokyo, Hiroshima, Saitama, Kanazawa, SLAC

1988-1992

Astro-E2 HXD & Integral

HXD-II has much narrower FOV and thus Background is lower and the sensitivity is higher.

SIGMA

OSSE

SPI

JEM-X

IBISHXDTobs =105s

COMPTEL

Continuum Sensitivities for HXD and INTEGRAL

CGRO/INTEGRALTobs = 106s

Continuum Spectrum

Simultaneous observation with highly sensitiveX-ray instruments gives us very unique opportunities to study gamma-ray sources.

High Resolution Detector (XRS) on AstroE2

kT (keV)

Direct measure of gas temperature

6 8 12eV

(Inoue, 2002)

Detection of a thermal Doppler width of an iron K-line:

for kT=10 keV, Eline=6.7 keV σL = 2.9eVand the intrinsic line width is 6.9 eV:

if we have 6 eV resolution…

200

150

100

50

0

Cou

nts

59105900589058805870Energy [eV]

FWHM: 5.93 ± 0.16 eV

GSFC

• Bulk motions of ICM in cluster mergers will be detected for the first time

Glast Mission

•International Mission •Japanese Contribution (Hiroshima,ISAS, RIKEN, Titech)• Wide FOV, Survey Operatiom• 20MeV - 300 GeV• Large Area Silicon Strips.

GLAST Large Area Telescope (LAT)

Burst Monitor (GBM)

Utilize Pair-productionSLAC

Tracker Module Mechanical Design

Carbon thermal panel

Bias supply

C-fiber face shee

Hex cell core

Al closeout

C-fiber face sheet

converter

4×4 array of Si-strip sensors (X)

Readout circuit 4×4 array of Si-strip　sensors (Y)

16 Towers

１５cm

by　Hiroshima Univ.

New approach GLAST will bring forth

- EGRET’s 3rd Catalog in 2 days -

100 sec

1 orbit**

1 day^̂

*zenith-pointed, ^“rocking” all-sky scan

All 3EG sources + ~ 80 new in 2 days

- GRB940217 (100sec)- PKS 1622-287 flare- 3C279 flare- Vela Pulsar

- Crab Pulsar- 3EG 2020+40 (SNR g Cygni?)

- 3EG 1835+59- 3C279 lowest 5s detection- 3EG 1911-2000 (AGN)- Mrk 421- Weakest 5s EGRET source

Time Variability Monitoring: Flares (Blazars, AGNs, Coronas), Precessions and Glitches (Pulsars), Lensing (AGNs)

Sensitvity of GLAST

CygnusRegion

3C279

Geminga

Vela

Cosmic RayInteractionsWith ISM

LMC

PKS 0528+134

PKS 0208-512

Crab

PSR B1706-44

CGRO-EGRET (1991-2000)

GLAST

NASA

Unidentified Source172 of the 271 sources in the EGRET 3rd catalog are “unidentified”

Cygnus region (15x15 deg)

EGRET source position error circles are ~0.5°, resulting in counterpart confusion.

GLAST will provide much more accurate positions, with ~30 arcsec -~5 arcmin localizations, depending on brightness.

From presentaion by S.Ritz, 20

Bright

Faint10 keV 30 MeV

Integral IBIS2002-

Glast2002-

CGRO-EGRET1989-2000

CGRO-COMPTEL1989-2000 Integral SPIE

2002-

Integral JEM-X2002-

ASCA/Astro-E

subMeV/MeV Gamma

Energy

Hard X-rays

Future Perspectives

Sensitivity Gap

Future Mission-- Focusing Hard X-ray Experiments --

ExtensibleOpticalBench

ISAS, JapanConstellation X

NASA

Focusing Telescope is not only for the equipment to take picturesbut also for the key to achieve high sensitivity.Because,a mirror concentrates the incoming flux onto a small spot of the detector, greatly reduce background.

ISAS’s “NeXT” mission

80 keV~800cm2 at 40keV

Key technology: Super Mirror & γ-ray Imager

NeXT Mission

These sensitivities are calculated for the case of the propobased on a CdTe pixel detector (HXI detector team, 2003)

Ein

E1

E2

electron

photon

θ

cosθ =1−mec

2

E1

+mec

2

E1 + E2

総重量1000 kg

COMPTEL(1989-2000)

Beyond COMPTEL

MEGA Mission (proposed by COMPTEL Team)

Compton-DominantRegion

COMPTEL has an effective area of ONLY 30̃40 cm

2

Weight 650kg

Next generation Compton Telescope in Japan

• Semiconductor Multi Compton Telescope (SMCT) (ISAS) 25cm

80layers

Compact BUT Detection Efficiency at 1 MeVbecomes 10 times higher thanCOMPTEL (weight 1 ton) on CGRO

80 layers of 0.5 mm thickCdTe strip detectors625 cm2 ×4cmCdTe Detector:

with high Z semiconductor (CdTe)

ISAS/SLAC/Osaka U. Hiroshima U./ U.Tokyo

Takahashi et al. SPIE 200

• Compton telescope based on Micro Gas Pixel Chamber(Kyoto Univ.)

Polarization• Polarization in X-ray/Gamma-rayis the only remaining parameter to be measured.• Expected from Jet Sources/Pulsars/Accretion Disk/GRB• Development of New and Sensitive Instruments are crucia

Gamma-rayby Newly Desined Gamma-ray Polarimeter(Kamae et al. 2003)

by Compton Telescope

(INTEGRAL, SMCT, MEGA…

Summary• X-ray and Gamma-ray energy band in

space are very important window to study high energy particles (cosmic rays) in the universe

• By combining information from X-ray and Gamma-ray observations, we can deepen our understandings of “Accelerator” in the universe